Regarding the binary neutron star system case, we considered the scenario of a very heavy component neutron star, in agreement with the recent observation of GW190814 event [1]}. Especially, we consider a heavy mass of \(m_1=2.59\; M_\odot \)  and we let the second star to fluctuate within the range \(m_2\in (1,2.59)\;M_\odot \) . By subtracting the component masses \(m_1, m_2\)  in Eq. (REF ) we obtain the corresponding range for the values of \(\mathcal {M}_c\) . Since the masses are defined, from the Eqs. (REF ) and (REF ), the effective tidal deformability \(\tilde{\Lambda }\)  can be determined.
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